The emergence of satellite missions that carried out long-term monitoring of stellar oscillations through their variation in luminosity with high-precision, such as Kepler [1]} and CoRoT [2]}, has opened a new window to estimate the mass of a large number of red giant stars [3]}, [4]}, [5]}, [6]}, [7]}, [8]}, [9]}, [10]}, which is otherwise almost inaccessible [11]}, [12]}, [13]}, [14]}.
Stars with a thick convective envelope show a particular type of oscillations (solar-like oscillations), which can be used to infer their structure including the mass [15]}, [16]}.
Having the mass of a red giant is of paramount importance in estimating its age since the time spent on the red giant branch is short compared to that on the main-sequence phase and since the mass is the fundamental parameter that controls the evolution of a star including its main-sequence lifetime, although mapping into an age scale is problematic since it depends on the adopted stellar models and assumed mass-loss [17]}.
Since red giants are intrinsically luminous, the development of asteroseismology allows us to explore stellar ages over a wide volume in the Galaxy.
These stellar ages obtained through asteroseismology have revealed the evolution of the Galactic disk [17]}, [19]}, [20]}, [21]}, [22]}.
